1. Thoughts on crab cavity noise, Fritz Caspers, 26.02.2008 Bandwidth of cavity structure with loaded Q is nearly always MUCH higher than generator bandwidth. Typically 3 db generator bandwidth ~1 Hz and -60 db points (phase noise down to -60 dBc =-60 db below carrier) are ~10 to 100 Hz away. Unless mechanical vibration (Lorentz forces) phase noise & jitter properties entirely determined by generator. “Phase noise” of the beam itself (synchrotron spectrum) is ALWAYS many orders of magnitude bigger than the phase noise of the generator. Phase noise can easily be converted into jitter (one can find nice interactive applets for this on the web: http://www.jittertime.com/resources/pncalc.shtml ) http://www.jittertime.com/resources/pncalc.shtml

2. Turn to turn jitter makes a huge difference wrt global jitter where you assume a infinitely stable reference source AND an infinite integration time. In the frame of turn to turn jitter the synchrotron motion is still visible but due to low synchrotron frequency it converts into very small time jitter numbers (short integration time) There is not only time jitter but also amplitude jitter (AM noise as compared to phase noise) and AM-PM as well as PM- AM conversion. As well known from BTF measurements, excitation of beam with frequencies inside the particle distributions can lead to blowup. But we can also excite the beam in the imaginary part of the BTF (just at the edge of the particle distribution) and virtually have no blowup. Certain analogies to stochastic cooling systems → consider experimental verification with existing stoch. cooling systems. In particular to check the claimed sensitivity to very small jitter effect

3. If the crab cavity concept (with kick and antikick) is really that delicate wrt timing drift and jitter( a few femto seconds) (how about amplitude noise?) then it is from my point of view not robust enough to be used in this way. But I have doubts that this is true … thus we need practical experiment to check the validity of this..apply your formulae to londitudinal stochastic cooling(simple filter method) and make some predictions….there we do have practical experience on hadron beams..or we could do some MD in the AD in summer. If it turns out to be true (i.e. if timing is really that delicate) then we can probably work around it, instead of operating the crab cavity exactly at the revolution harmonic we can use instead two sine waves (simultaneously) one slightly above and the other slightly below n x Frev.(in the same cavity just taking advantage of the 3 db bandwith and the finite loaded Q of the cavity)

4. The price to be paid would be an envelope having an amplitude modulation of Delta F, (more precisely : amplitude modulation with suppressed carrier)i.e. a time dependent crabbing but in the worst case this cost a factor of 2 in crabbing efficiency and may have other benefits. Then we can set those two frequencies precisely in the imag part of the longitudinal BFT and this way get many orders of magnitude less blowup as compared to working with a single sinewave in the center. Last thought: crab cavity affects transverse phase space, but sits on longitudinal revolution harmonic ; therefore it should not cause any transverse blowup, since its frequency is far from the transverse Schottky bands, or only longitudinally via second order effects

5. LHC upgrade scenarios emerging from CARE-HHH workshops IR’07 Frascati BEAM’07 CERN LHC-LUMI-06 Valencia LHC-LUMI-05 Arcidosso HHH-2004 CERN ↑ F. Ruggiero, W. Scandale, J.-P. Koutchouk, L. Evans, LARP, F. Zimmermann

6. Name Event Date Name Event Date6 LHC upgrade path 1: early separation (ES) ultimate LHC beam (1.7x10 11 protons/bunch, 25 spacing) ultimate LHC beam (1.7x10 11 protons/bunch, 25 spacing) squeeze  * to ~10 cm in ATLAS & CMS squeeze  * to ~10 cm in ATLAS & CMS add early-separation dipoles in detectors starting at ~ 3 m from IP add early-separation dipoles in detectors starting at ~ 3 m from IP possibly also add quadrupole-doublet inside detector at ~13 m from IP possibly also add quadrupole-doublet inside detector at ~13 m from IP and add crab cavities (  Piwinski ~ 0) and add crab cavities (  Piwinski ~ 0) → hardware inside ATLAS & CMS detectors, first hadron crab cavities; off-  ultimate bunches + near head-on collision stronger triplet magnets D0 dipole small-angle crab cavity optional Q0 quad’s J.-P. Koutchouk

7. Name Event Date Name Event Date7 LHC upgrade path 2: full crab crossing (FCC) ultimate LHC beam (1.7x10 11 protons/bunch, 25 spacing) ultimate LHC beam (1.7x10 11 protons/bunch, 25 spacing) squeeze  * to ~10 cm in ATLAS & CMS squeeze  * to ~10 cm in ATLAS & CMS and add crab cavities with 60% higher voltage than for ES (  Piwinski ~ 0) and add crab cavities with 60% higher voltage than for ES (  Piwinski ~ 0) → first hadron crab cavities, off-  -beat ultimate bunches + near head-on collision stronger triplet magnets small-angle crab cavity L. Evans, W. Scandale, F. Zimmermann

8. Name Event Date Name Event Date8 LHC upgrade path 3: large Piwinski angle (LPA) double bunch spacing to 50 ns, longer & more intense bunches with  Piwinski ~ 2 double bunch spacing to 50 ns, longer & more intense bunches with  Piwinski ~ 2  *~25 cm, do not add any elements inside detectors  *~25 cm, do not add any elements inside detectors long-range beam-beam wire compensation long-range beam-beam wire compensation → novel operating regime for hadron colliders, beam generation fewer, long & intense bunches + nonzero crossing angle + wire compensation wire compensator larger-aperture triplet magnets F. Ruggiero, W. Scandale. F. Zimmermann

9. parametersymbolnominalultimateEarly Sep.Full Crab XingL. Piw Angle transverse emittance  [  m] 3.75 protons per bunchN b [10 11 ] 1.15 1.7 4.9 bunch spacing  t [ns] 25 50 beam currentI [A] 0.58 0.86 1.22 longitudinal profile Gauss Flat rms bunch length  z [cm] 7.55 11.8 beta* at IP1&5  [m] 0.55 0.50.08 0.25 full crossing angle  c [  rad] 285 31500381 Piwinski parameter  c  z /(2*  x *) 0.64 0.75002.0 hourglass reduction 1 2.30.86 0.99 peak luminosityL [10 34 cm -2 s -1 ] 19 4415.5 10.7 peak events per #ing 22 14294 403 initial lumi lifetime  L [h] 0.46 0.912.2 4.5 effective luminosity (T turnaround =10 h) L eff [10 34 cm -2 s -1 ] 21.2 17.02.4 2.5 T run,opt [h] 0.56 1.156.6 9.5 effective luminosity (T turnaround =5 h) L eff [10 34 cm -2 s -1 ] 15.0 12.03.6 3.5 T run,opt [h] 1.07 (0.44) 1.04 (0.59)4.6 6.7 e-c heat SEY=1.4(1.3)P [W/m] 0.17 0.251.04 (0.59) 0.36 (0.1) SR heat load 4.6-20 KP SR [W/m] 0.15 0.330.25 0.36 image current heatP IC [W/m] 0.04 (0.38) 0.06 (0.56)0.33 0.78 gas-s. 100 h (10 h)  b P gas [W/m]4.54.30.06 (0.56) 0.09 (0.9) extent luminous region  l [cm] 3.7 5.3 comment nominalultimateD0 + crab crabwire comp. large Piwinski angle (LPA) full crab crossing (FCC) early separation (ES)

10. for operation at beam-beam limit with alternating planes of crossing at two IPs ↓↓ ES/FCC ↑↑ LPA ↓ LPA where (  Q bb ) = total beam-beam tune shift; ↑ LPA↓ ES/FCC peak luminosity with respect to ultimate LHC (2.4 x nominal): ES or FCC: x 6 x 1.3 x 0.86 = 6.7 ↑ ES/FCC LPA: ½ x2 x2.9x1.3 x1.4 = 5.3 ↑ LPA what matters is the integrated luminosity

11. ring impedance crab frequency beam parameters cryogenics noise crab wake fields space aperture rf generator cavity design beam tests optics collimation magnets interrelations beam-beam low-level RF LHC upgrade plan → global effort